ArcAdiAThe DSpace digital repository system captures, stores, indexes, preserves, and distributes digital research material.http://dspace-roma3.caspur.it:802015-03-04T00:11:12Z2015-03-04T00:11:12ZVariable partial covering and a relativistic iron line in NGC 1365Risaliti, GuidoMiniutti, GiovanniElvis, MartinFabbiano, GiuseppinaSalvati, MarcoBaldi, AlessandroBraito, ValentinaBianchi, StefanoMatt, GiorgioReeves, JamesSoria, RobertoZezas, Andreashttp://hdl.handle.net/2307/2952011-12-22T13:34:55Z2009-04-30T22:00:00Z<Title>Variable partial covering and a relativistic iron line in NGC 1365</Title>
<Authors>Risaliti, Guido; Miniutti, Giovanni; Elvis, Martin; Fabbiano, Giuseppina; Salvati, Marco; Baldi, Alessandro; Braito, Valentina; Bianchi, Stefano; Matt, Giorgio; Reeves, James; Soria, Roberto; Zezas, Andreas</Authors>
<Issue Date>2009-05-01</Issue Date>
<Is part of>Astrophysical Journal</Is part of>
<Volume>696</Volume>
<Pages>160-171</Pages>
<Abstract>We present a complete analysis of the hard X-ray (2-10 keV) properties of the Seyfert galaxy NGC 1365, based on a 60 ks XMM-Newton observation performed in 2004 January. The two main results are as follows. (1) We detect an obscuring cloud with N-H similar to 3.5 x 10(23) cm(-2) crossing the line of sight in similar to 25 ks. This implies a dimension of the X-ray source not larger than a few 1013 cm and a distance of the obscuring cloud of the order of 1016 cm. Adopting the black hole mass M-BH estimated from the M-BH-velocity dispersion relation, the source size is D-S < 20R(G) and the distance and density of the obscuring clouds are R similar to 3000-10,000R(G) and n similar to 10(10) cm(-3), i.e., typical values for broad-line region clouds.(2) An iron emission line with a relativistic profile is detected with high statistical significance. A time-integrated fit of the line+continuum reflection components suggests a high iron abundance(approximately three times solar) and an origin of these components in the inner part (within similar to 10R(G)) of the accretion disk, in agreement with the small source size inferred from the analysis of the absorption variability.</Abstract>2009-04-30T22:00:00ZThe XMM-Newton long look of NGC 1365: uncovering of the obscured X-raysourceRisaliti, GuidoSalvati, MarcoElvis, MartinFabbiano, GiuseppinaBaldi, AlessandroBianchi, StefanoBraito, ValentinaGuainazzi, MatteoMatt, GiorgioMiniutti, GiovanniReeves, JamesSoria, RobertoZezas, Andreashttp://hdl.handle.net/2307/3052011-12-22T13:34:34Z2008-12-31T23:00:00Z<Title>The XMM-Newton long look of NGC 1365: uncovering of the obscured X-raysource</Title>
<Authors>Risaliti, Guido; Salvati, Marco; Elvis, Martin; Fabbiano, Giuseppina; Baldi, Alessandro; Bianchi, Stefano; Braito, Valentina; Guainazzi, Matteo; Matt, Giorgio; Miniutti, Giovanni; Reeves, James; Soria, Roberto; Zezas, Andreas</Authors>
<Issue Date>2009</Issue Date>
<Is part of>Monthly notices of the royal astronomical society</Is part of>
<Volume>393</Volume>
<Pages>L1</Pages>
<Abstract>We present an analysis of the extreme obscuration variability observedduring an XMM-Newton 5-d continuous monitoring of the active galacticnuclei (AGN) in NGC 1365. The source was in a reflection-dominatedstate in the first similar to 1.5 d, then a strong increase in the 7-10keV emission was observed in similar to 10 h, followed by a symmetricdecrease. The spectral analysis of the different states clearly showsthat this variation is due to an uncovering of the X-ray source. Fromthis observation, we estimate a size of the X-ray source D-S < 10(13)cm, a distance of the obscuring clouds R similar to 10(16) cm and adensity n similar to 10(11) cm(-3). These values suggest that the X-rayabsorption/reflection originates from the broad-line region clouds.This is also supported by the resolved width of the iron narrow K alphaemission line, consistent with the width of the broad H beta line.</Abstract>2008-12-31T23:00:00Z